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Astrophysical Bulletin, vol. 63, No.3, 2008, pp.278-289 Translated from Astrofizicheskij Byulleten, vol.63, No.3, 2008, pp. 298-310

September 3, 2008

Speckle Interferometry of Metal-Poor Stars in the Solar Neighborhood. II
D. A. Rastegaev, Yu. Yu. Balega, A. F. Maksimov, E. V. Malogolovets, V. V. Dyachenko
Sp ecial Astrophysical Observatory, RAS, Nizhnii Arkhyz, Karachai-Cherkessian Republic, 357147 Russia received: April 7, 2008/revised: April 21, 2008 Abstract. The results of sp eckle interferometric observations of 115 metal-p oor stars ([m/H] < -1) within 250 p c from the Sun and with prop er motions µ 0.2 /yr, made with the 6-m telescop e of the Sp ecial Astrophysical Observatory of the Russian Academy of Sciences, are rep orted. Close companions with separations ranging from 0.034 to 1 were observed for 12 ob jects -- G76-21, G59-1, G63-46, G135-16, G168-42, G141-47, G142-44, G19010, G28-43, G217-8, G130-7, and G89-14 -- eight of them are astrometrically resolved for the first time. The newly resolved systems include one triple star -- G190-10. If combined with sp ectroscopic and visual data, our results imply a single:binary:triple:quadruple star ratio of 147:64:9:1 for a sample of 221 primary comp onents of halo and thick-disk stars.

arXiv:0809.0575v1 [astro-ph] 3 Sep 2008

1. INTRODUCTION
Metal-poor stars of the Galactic halo and thick disk bear important information about the chemical and kinematical properties of matter at the epoch of the formation of the Milky Way. Of special importance is the study of the orbital parameters of binary and multiple systems, which provide a source of data on stellar masses and luminosities. To estimate the fraction of multiple stars and determine the orbital parameters of old metal-poor stars, we started a speckle interferometric survey of such ob jects located within 250 pc from the Sun. Rastegaev et al. (2007) described a sample of 223 population-II dwarf stars in the solar neighborhood and reported the results of the survey of the first 109 stars of the sample performed with the 6 m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS). The sample includes nearby F, G, and early K-type subdwarfs down to 12th magnitude in the V band (Fig. 1) with metalicities [m/H] < -1 and proper motions µ 0.2 /yr (Fig. 2). In this paper we continue to report the results of speckle interferometric observations for the remaining 114 stars of the halo and thick disk performed with the 6 m telescope of the SAO RAS in 2007. We also report the results of repeated speckle-interferometric observations of our earlier resolved subsystem of the quadruple star G89-14 (Rastegaev et al., 2007).

Fig. 1. Distribution of the V -band magnitudes of stars of the sample studied.

2. OBSERVATIONS
The speckle-interferometric observations were performed with the 6 m telescope of the of the SAO RAS in March (52 ob jects), June­July (52 ob jects), and September (10 ob jects), 2007. In addition, we also reobserved in two filters the interferometric subsystem of the quadruple star G89-14 that we discovered in December, 2006 (Rastegaev et al., 2007). In September we observed six objects resolved in June and July (G141-47, G142-44, G2178, G130-7,G190-10, and G28-43). We also reobserved the unresolved ob jects G183-9, G24-17, G26-1, and G128-11 in order to obtain their power spectra with higher signalto-noise ratio.

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Rastegaev et al.: Sp eckle Interferometry of Metal-Poor Stars .I I

for the component magnitude difference, separation, and position angle, respectively.

3. RESULTS OF OBSERVATIONS
Table 1 lists the resolved stars. We observed the speckleinterferometric components for 12 ob jects, one of them is the quadruple system G89-14, which was resolved for the first time in December, 2006 (Rastegaev et al., 2007). We were the first to astrometrically resolve eight (G7621, G135-16, G141-47, G142-44, G190-10, G28-43, G2178, and G130-7) of the 11 remaining systems. Among the new systems we point out G190-10, where we discovered the third component in the earlier known spectroscopic binary (Latham et al., 2002). In addition to new observations, we also report the results of our re-reduction of stars from (Rastegaev et al., 2007) (Table 2). Our new results for these stars slightly differ from those reported in our previous paper (Rastegaev et al., 2007) by corrected estimates of angular separations due to the refined coefficients of the transition from pixel measurements to angular units. It goes without saying that these corrections have appreciable effect only for wide pairs. In addition, we also thoroughly analyzed the measurement errors for each ob ject and, in contrast to our earlier paper (Rastegaev et al., 2007), give the epoch of observation for each individual pair. We list the so far unresolved stars in Table 3.

Fig. 2. Distribution of the proper motions of the stars of the sample. For better visualization, we do not show in the histogram the star G122-51 with anomalously high proper motion (µ = 7.042 /yr).

In our observations we use a facility based on EMCCD (a 512в512 CCD with internal electron gain), which has high quantum efficiency and linearity, allowing ob jects to be discovered with component magnitude differences m 5 at the diffraction-limited resolution of the telescope. The size of the detector field (4.4 ) allowed secondary components to be discovered at separations as large as 3 from the primary star. We recorded the speckle interferograms in three filters: 550/20, 600/40, and 800/100 nm (the numbers indicate the central transmission wavelength of the filter and the transmission bandwidth, respectively) with exposures ranging from 5 to 20 milliseconds. We took 2000 images in each filter for almost all the ob jects observed in March and 1940 exposures for every ob ject observed in June, July, and September. Weather conditions during March set were not favorable for speckle-interferometric observations (seeing was at about 3 ). During the June and September observations, on the contrary, seeing was (1.0 - 1.5) , and sometimes even better than 1 . We calibrated our measurements using the so-called "standard" pairs--binaries with well-known component separations and position angles. In addition, in September we used an opaque mask with a pair of circular holes, which was located in the beam converging from the primary mirror of the telescope, to calibrate the scale and position angle. The known geometry of the holes allows the image scale and angular orientation of the CCD to be determined in each filter from the fringe pattern. In this method we used Deneb as the bright source. Descriptions of the technique that we used to determine the relative positions and component magnitude differences of the ob jects studied from speckle interferograms averaged over a series of power spectra can be found in Balega et al. (2002) and Pluzhnik (2005). The accuracy of this technique may be as good as 0.02m , 0.001, and 0.1

4. SUPPLEMENTARY DATA FOR RESOLVED STARS
In this section we gather the supplementary data on resolved stars (see also Table 4). For some of the ob jects we give two distances inferred from trigonometric (Perryman, 1997) and photometric (Carney et al., 1994) parallaxes. The latter distance is evidently underestimated, because it does not take the additional component into account. On the other hand, the additional component also contributes to the error of the measured trigonometric parallax, especially in short-period systems. G76-21 (02h 41m 13s 6 +09 46 12 ; HIP 12529). It is . an F2-type star (SIMBAD database) at a heliocentric distance of about 190 pc (Perryman, 1997) or 90 pc according to Carney et al. (1994). The star was observed using the method of lunar occultations, but it was not resolved into individual components (Richichi & Percheron, 2002). It is known as a suspected SB2 system based on the results of metallicity measurements (Carney et al., 1994). Spectroscopic observations of this star show signs of about 10-day periodicity, however, no conclusive evidence could be found for radial-velocity variations (Latham, 2008). We were the first to astrometrically resolve this star. G89-14 (07h 22m 31s 5 +08 49 13 ; HIP 35756; . WDS 07224+0854). We earlier discovered the fourth


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component (Rastegaev et al., 2007) in the triple system consisting of a spectroscopic binary with a period of 190 days (Latham et al., 2002) and a common proper-motion companion at an angular separation of 34 from this binary (Allen et al., 2000). Repeated observations in the 550/20 filter failed to reveal the speckle interferometric component at a distance of 0.98 from the spectroscopic pair, because in this part of the spectrum the component in question is 5m fainter than the SB1 pair. Observations in the 800/100 filter (see Table 1) performed in March, 2007, confirmed the results of the December, 2006 observations to within the quoted errors. The heliocentric distance of the quadruple system is equal to 95 pc (Carney et al., 1994) or to about 170 pc according to (Perryman, 1997). G59-1 (12h 08m 54s 7 +21 47 19 ; HIP 59233; . WDS 12089+2147). It is a triple system. The inner pair, which has an integrated spectral type of G2V(SIMBAD database) was discovered by HIPPARCOS (Perryman, 1997). The outer component, which is located at an angular distance of about 16 , has common proper motion with the inner pair (Allen et al., 2000). We resolved the inner subsystem. The heliocentric distance is equal to about 110 pc (Perryman, 1997) or 50 pc according to (Carney et al., 1994). G63-46 (13h 39m 59s 6 +12 35 22 ; . HIP 66665; WDS 13400+1235). A double star of spectral type F9V (SIMBAD database) was first resolved by the HIPPARCOS satellite (Perryman, 1997) and measured speckle interferometrically by Zinnecker et al. (2004) and Hartkopf et al. (in preparation). The heliocentric distance of the system is equal to about 130 pc (Perryman, 1997) or 60 pc (Carney et al., 1994). G135-16 (14h 04m 01s 6 +2231 30 ; HIP 68714). A . double star of spectral type G2 (SIMBAD database). This pair, which we astrometrically resolved for the first time, must be an SB1 type spectral binary with a period of 2606 days (Latham et al., 2002). Its estimated heliocentric distance is about 80 pc (Perryman, 1997) or 65 pc (Carney et al., 1994). G168-42 (16h 19m 51s 7 . +22 38 20 ; HIP 80003). An astrometric binary (Zinnecker et al., 2004, Law et al., 2006) of spectral type sd:G2 (SIMBAD database). We are the first to report the component magnitude difference for this system. Latham et al. (2002) list it as a spectroscopic binary with unknown period. The star exhibits a systematic decrease of radial velocity over more than 24 years of its spectroscopic observations(Latham, 2008). Its heliocentric distance is about 110 pc (Perryman, 1997) or 100 pc (Carney et al., 1994) if inferred from the trigonometric or photometric parallax, respectively. G141-47 (18h 53m 16s 5 +10 37 26 ; BD+10 3711 . TYC 1030-316-1). This first resolved pair with an angular separation of about 0.04 is an SB1 spectroscopic binary with a period of 388.52 days (Latham et al., 2002) and a spectral type of F8 (SIMBAD database). We may

have discovered the third component in the known spectroscopic pair. The heliocentric distance to this ob ject is 110 pc (Carney et al., 1994). The system was observed twice in June in the 550/20 and 800/100 filters, and also in September in the 800/100 filter. In Table 1 we give only the preliminary photometry of the speckle interferometric pair based on the results of the June observations in the 800/100 filter due to the low signal-to-noise ratio of the integrated power spectra. G142-44 (19h 38m 53s 2 +16 25 34 ; NLTT 48059; . TYC 1602-2423-1). This first resolved G5-type binary is located at a heliocentric distance of 110 pc (Carney et al., 1994). We observed this pair four times (see Table 1), and three of them in the 800/100 filter. The weak fringe contrast in the power spectrum in the 600/40 filter allowed only the lower boundary of component magnitude difference to be estimated in this part of the spectrum. G190-10 (23h 07m 59s 8 +41 51 20 ; NLTT 55914; . TYC 3224-2564-1). A new triple system of spectral type G1 (SIMBAD database). We found the third, outer component at an angular distance of 0.98 from this earlier known SB1 system with a period of 30 days (Latham et al., 2002). The ob ject is located at a distance of 90 pc (Carney et al., 1994). G28-43 (23h 09m 32s 9 +0042 40 ; HIP 114349). A . binary of the spectral type G2 (SIMBAD database), which we resolved for the first time. The ob ject is located at a distance of 40 pc (Carney et al., 1994). The HIPPARCOS catalog lists no parallax for the system (SIMBAD database). The wide component CCDM J23096+0043B at an angular separation of 12.2 does not form a physical pair (Zapatero Osorio & Martin, 2004). G217-8 (23h 26m 32s 8 +60 37 43 ; HIP 115704). We . were the first to astrometrically resolve this F2-type spectroscopic binary (SIMBAD database) with a preliminary orbit (9632 days period) (Latham et al., 2002). The distance to the system is equal to about 110 pc (Perryman, 1997) or 105 pc (Carney et al., 1994). We observed the ob ject twice: in June, in the 600/40 filter and in September, in the 800/100 filter. Unfortunately, the insufficient quality of the power spectra in both filters did not make it possible to determine the component magnitude difference and showed up in the accuracy of the inferred positional parameters (see Table 1). G130-7 (23h 45m 00s 1 +3020 10 ; HIP 117150). An F. type system (SIMBAD database) at a distance of about 160 pc (Perryman, 1997) (or 120 pc from other data (Carney et al., 1994)), which was resolved for the first time.

5. MULTIPLICITY OF STARS 5.1. Distant Comp onents
We use the additional available data on spectroscopic multiplicity (Goldberg et al., 2002, Latham et al., 2002) and distant components from the WDS (Mason et al., 2001)


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Rastegaev et al.: Sp eckle Interferometry of Metal-Poor Stars .I I

for the 114 ob jects studied. Whereas spectroscopic and interferometric measurements provide conclusive evidence indicating that the components in question are physically bound, wide visual components should be treated with more care. We found a total of 104 WDS companions for our stars and discarded most of them as optical pro jections. Table 5 lists the data for all the wide components found for the stars of our sample. Column 1 gives the names of the stars studied; column 2--all the WDS components found for the star. For the components found to be physically bound to the stars of the sample columns 3 and 4 list the angular separation (in arcsec) and magnitude difference, respectively. Column 5, which is entitled "Status", indicates the components that we consider to be physically bound with the primary star ("+") and optically pro jected (unbound) pairs ("-"). The additional question mark in this column indicates that we are not certain about the adopted decision, nd a single question mark indicates that only a single measurement is available, which does not allow any conclusions concerning the physical bound between the components. The last column gives the references to the papers containing the data on the corresponding pair and whether the physical association between the components is confirmed or disproved. These are in all cases the papers of Allen et al. (2000) and Zapatero Osorio & Martin (2004) dedicated to wide pairs of population-II stars and the HIPPARCOS catalog (Perryman, 1997). The additional symbol in this column indicates that our observations confirm the presence of the component considered. In cases with no references given we made decision concerning the physical boundness on our own, based on the data listed in the WDS catalog. To this end, we analyzed the variations of component separations and magnitude differences with time. As a result, we left only seven WDS components (marked "+" or "+?") of 104, and took them into account when counting the number of systems of different multiplicity.

parameters is available for this star, which does not allow any conclusions be made for it. We added two unaccounted binaries BD+25 1981 and HD97916 from (Carney et al., 2001), and assumed the three systems-- G43-3 (see also (Carney et al., 2001)), G186-26, and G210-33 to be binaries based on the small variation of radial velocities (Latham, 2008). As a result, the single:binary:triple:quadruple ratio for the 221 primary-component halo and thick-disk stars (Rastegaev et al., 2007) discovered using all methods is equal to 147:64:9:1. Thus out of 306 stars considered-- 223 observed stars and 83 their satellites--more than a half (159) belong to multiple systems. The multiplicity of the sample--i.e., the ratio of the number of multiple systems to the total number of systems--is about 33%. Duquennoy & Mayor (1991) obtained a similar estimate for disk stars of spectral types ranging from F7 to G9 and found it to be 51:40:7:2. We point out the difference between the two samples compared. Whereas we constructed our sample by selecting stars with certain magnitudes and space velocities, the sample of Duquennoy and Mayor is only distance limited: all their stars are located within 22 pc from the Sun.

6. CONCLUSIONS
The speckle interferometric survey of 223 metal-poor stars from the solar neighborhood was performed with the 6 m telescope of the Special Astrophysical Observatory. Nineteen binary and multiple systems were resolved. From these, 15 ob jects were resolved astrometrically for the first time. Three of our resolved systems--G76-21 (HIP 12529), G114-25 (HIP 44111), and G217-8 (HIP 115704) have metallicities [m/H] < -2 (Carney et al., 1994). The additional data on the spectroscopic (Goldberg et al., 2002; Latham et al., 2002; Carney et al., 1994; Carney et al., 2001) and astrometric (Mason et al., 2001; Zapatero Osorio & Martin, 2004; Allen et al., 2000) multiplicity allowed us to estimate the single:binary:triple:quadruple star ratio to be 147:64:9:1. Part of the speckle interferometric pairs with relatively short periods are suitable for monitoring in order to compute their orbits and determine the masses of metal-poor stars, which are necessary for the calibration of the mass­ luminosity relation. Such studies are of great importance, because even now we badly lack the empirical data for the metallicity interval considered. The sample presented in (Rastegaev et al., 2007) is the most thoroughly analyzed one in terms of the multiplicity of halo and thick-disk stars. This circumstance allows the sample to be used for statistical studies where physically bound components play important part. One must bear in mind the selection effects due to heliocentric distances to the ob jects, their multiplicity and proper motions. An addition, low-mass companions could be missed for the stars of survey because of limitations of the methods. All this must stimulate further observations and theoretical studies.

5.2. Ratio of systems of different multiplicity
We computed the ratio of systems of different multiplicity using all the published data on the observations of the corresponding systems using various methods. Of the 114 stars considered 27 are spectroscopic binaries (Goldberg et al., 2002; Latham et al., 2002; Carney et al., 1994) and 11 stars are speckle interferometric binaries. Seven stars have companions from the WDS catalog. When analyzing spectroscopic binaries we took into account both the pairs with known orbital periods and the systems for which no periods have been determined. It goes without saying that there exist components which can be found using several different methods. In addition, we also analyzed the ratio of systems of different multiplicity from Rastegaev et al. (2007). We excluded G120-15 from the list of binary stars, because only one measurement of the positional


Rastegaev et al.: Sp eckle Interferometry of Metal-Poor Stars .I I Acknow ledgements. This work was supp orted by the Russian Foundation for Basic Research (pro ject no. 04-02-17563) and the program of the Physical Sciences of the Russian Academy of Sciences. This research made use of the Simbad database and WDS (Mason et al., 2001) catalog. We are grateful to D.Latham for sharing the data on the sp ectroscopic multiplicity and orbital p eriods of selected ob jects.

5

References
C. Allen, A. Poveda and M. A. Herrera, A&A 356, 529 (2000). I. I. Balega, Y. Y. Balega, K.-H. Hofmann, et al., A&A 385, 87 (2002). B. W. Carney, D. W. Latham, J. B. Laird et al., AJ 107, 2240 (1994) (CLLA). B. W. Carney, D. W. Latham, J. B. Laird et al., AJ 122, 3419 (2001). A. Duquennoy and M. Mayor, A&A 248, 485 (1991). D. Goldb erg, T. Mazeh, D. W. Latham et al., AJ 124, 1132 (2002). W. I. Hartkopf, B. D. Mason, and T. Rafferty, (in preparation). D. W. Latham, R. P. Stefanik, G. Torres et al., AJ 124, 1144 (2002). D. W. Latham, p ersonal communication (2008). N. M. Law, S. T. Hodgkin, and C. D. Mackay, MNRAS 368, 1917 (2006). B. D. Mason, G. L. Wycoff, W. I. Hartkopf et al., AJ 122, 3466 (2001). M. A. C. Perryman, ESA, The Hipparcos and Tycho Catalogues (ESA Publ. Division, SP­1200, 1997). E. A. Pluzhnik, A&A 431, 587 (2005). D. A. Rastegaev, Yu. Yu. Balega, E. V. Malogovets, AstBu 62, 251 (2007). A. Richichi, I. Percheron, A&A 386, 492 (2002). SIMBAD database: http://simbad.u-strasbg.fr/simbad/sim-fid M. R. Zapatero Osorio and E .L. Martin, A&A 419, 167 (2004). H. Zinnecker, R. Kohler, and H. Jahreiss, Rev. Mex. A & A 21, 33 (2004).


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Table 1. Results of the speckle-interferometric measurements for resolved ob jects
Name of the ob ject G76-21 G89-14 G59-1 G63-46 G135-16 G168-42 G141-47 G141-47 G141-47 G142-44 G142-44 G142-44 G142-44 G190-10 G190-10 G190-10 G28-43 G28-43 G28-43 G217-8 G217-8 G130-7 G130-7 Other designation HIP 12529 HIP 35756 HIP 59233 HIP 66665 HIP 68714 HIP 80003 BD+10 3711 BD+10 3711 BD+10 3711 NLTT 48059 NLTT 48059 NLTT 48059 NLTT 48059 NLTT 55914 NLTT 55914 NLTT 55914 HIP 114349 HIP 114349 HIP 114349 HIP 115704 HIP 115704 HIP 117150 HIP 117150 Epoch 2007.73116 2007.24040 2007.24333 2007.24084 2007.24388 2007.24109 2007.48727 2007.48728 2007.73870 2007.49008 2007.49286 2007.49287 2007.73871 2007.51184 2007.73885 2007.73886 2007.51209 2007.51210 2007.73877 2007.49527 2007.72510 2007.51188 2007.73888 ( ) 206.4 0.8 280.5 82.9 174.8 208.0 143 139 137 193.2 192.9 193.3 287.0 286.9 286.9 37.6 37.4 37.7 263 260 230.0 230.7


( ) 0.047 0.982 0.098 0.222 0.034 0.180 0.041 0.034 0.044 0.661 0.663 0.665 0.977 0.982 0.982 0.425 0.425 0.424





m 0.4 4.3 1.4 0.94 0.7 1.34 0.9



m

/ 800/100 800/100 800/100 550/20 550/20 800/100 800/100 550/20 800/100 800/100 800/100 600/40 800/100 800/100 800/100 550/20 800/100 600/40 800/100 600/40 800/100 800/100 800/100

0.7 0.4 0.7 0.3 1.7 0.4 4 20 6 0.7 0.5 0.5 0.2 0.3 0.3 0.4 0.6 0.4 5 5 1.5 1.0

0.001 0.005 0.002 0.001 0.001 0.001 0.005 0.013 0.005 0.007 0.005 0.005 0.001 0.002 0.002 0.003 0.004 0.003 0.09 0.07 0.005 0.004

0.1 0.1 0.1 0.02 0.1 0.02 0.6

3.7 3.7 3.85 1.39 1.37 1.73 3.35 3.5 3.32 0.02 0.02 2.98 2.95

0.2 0.1 0.06 0.02 0.02 0.03 0.04 0.1 0.03

0.191 0.191

0.06 0.04

Table 2. Speckle-intermerometric measurements of ob jects resolved by Rastegaev et al. (2007)
Name of the ob ject G102-20 G191-55 BD+19 1185A G89-14 G87-45 G87-45 G87-47 G111-38AB G111-38AB G111-38AC G111-38AC G111-38BC G111-38BC G114-25 --the p osition of Other designation HIP 26676 BD+58 876 HIP 28671 HIP 35756 NLTT 18038 NLTT 18038 HIP 36936 HIP 38195 HIP 38195 HIP 38195 HIP 38195 HIP 38195 HIP 38195 HIP 44111 the secondary Epoch 2006.94164 2006.94475 2006.94711 2006.94455 2006.94723 2006.94724 2006.94725 2006.94751 2006.94749 2006.94751 2006.94749 2006.94751 2006.94749 2006.94742 comp onent is ( )


( ) 0.119 0.806 0.114 0.979 0.282 0.282 0.077 0.084 0.084 2.111 2.112 2.193 2.194 0.773 180 amb





m 3.2 2.00 1.77 4.1 2.01 1.76 1.7 0.78 0.75 1.34 1.10 0.57 0.36 3.9



m

/ 550/20 800/100 550/20 800/100 550/20 800/100 800/100 550/20 800/100 550/20 800/100 550/20 800/100 800/100

308.0 2.8 125.1 0.3 183.6 0.7 0.8 0.4 271.3 0.5 270.7 0.4 54.0 2.1 7.9 0.7 7.8 1.3 200.0 0.3 200.0 0.3 199.5 0.3 199.5 0.3 323.7 0.5 known with ±

0.006 0.007 0.002 0.009 0.004 0.003 0.003 0.002 0.002 0.018 0.018 0.019 0.019 0.008 iguity.

0.4 0.11 0.04 0.4 0.04 0.04 0.3 0.03 0.03 0.04 0.04 0.05 0.05 0.2


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7

Table 3. Unresolved stars
Name G265-1 G130-65 G31-55 HD 3567 G242-65 G242-71 G271-162 BD-1 306 G75-31 G4-36 G4-37 G75-56 G95-11 G89-14 G13-9 G11-44 G123-9 G12-21 G13-35 G13-38 G199-20 G59-27 G60-46 G60-48 G14-33 G177-23 G255-32 G62-52 G64-12 G150-40 G165-39 G65-22 G64-37 G239-12 G178-27 G201-5 G66-30 G166-54 G66-51 G179-22 G201-44 G15-24 G168-26 G180-24 G202-35 G180-58 G153-64 G17-25 G202-65 G180-66 G169-28 G139-8 G19-25 G139-49 Filter (/,nm) 550/20; 800/100 800/100 600/40; 800/100 600/40; 800/100 600/40 600/40 800/100 550/20; 800/100 800/100 800/100 800/100 800/100 800/100 550/20 550/20 550/20 800/100 550/20 550/20 550/20 800/100 800/100 550/20 550/20 800/100 550/20 800/100 550/20 800/100 800/100 550/20 800/100 800/100 800/100 550/20 800/100 550/20 800/100 550/20 550/20 550/20 800/100 800/100 550/20 800/100 800/100 800/100 550/20; 800/100 800/100 800/100 800/100 800/100 550/20 550/20 Epoch 2007.4952 2007.5147 2007.7253 2007.7254 2007.4953 2007.4952 2007.7391 2007.7391 2007.7312 2007.7312 2007.7312 2007.7366 2007.7367 2007.2404 2007.2406 2007.2406 2007.2464 2007.2406 2007.2406 2007.2406 2007.2465 2007.2464 2007.2407 2007.2407 2007.2408 2007.2465 2007.2466 2007.2435 2007.2436 2007.2464 2007.2464 2007.2463 2007.2409 2007.2466 2007.2464 2007.2435 2007.2410 2007.2409 2007.2410 2007.2465 2007.2435 2007.2466 2007.2410 2007.2434 2007.2435 2007.2434 2007.2438 2007.2438 2007.2435 2007.2435 2007.2412 2007.2411 2007.2494 2007.2494 Name G20-15 G182-31 G183-9 G183-9 G183-11 G182-32 G183-16 G20-24 G140-44 G140-46 G206-34 G21-19 G125-5 G92-6 BD+26 3578 HD 188510 G186-26 HD 194598 G262-14 G24-17 G24-17 G24-25 G210-33 G212-7 HD 201891 G25-24 G187-40 G26-1 G26-1 G126-10 G93-27 G231-52 G188-22 G126-36 G188-30 G232-40 G214-5 G27-8 G126-52 G126-62 LFT 1697 G18-39 G156-7 G18-54 G27-33 G233-26 G128-11 G128-11 G242-14 G68-3 G190-15 G29-25 G29-71 G20-8 Filter (/,nm) 550/20; 800/100 550/20 550/20 600/40 550/20 800/100 550/20 550/20; 800/100 550/20; 800/100 550/20; 800/100 800/100 550/20; 800/100 550/20 600/40; 800/100 550/20; 800/100 550/20; 800/100 600/40; 800/100 600/40 600/40; 800/100 600/40 800/100 800/100 800/100 550/20; 800/100 550/20; 800/100 800/100 800/100 600/40; 800/100 800/100 800/100 800/100 600/40; 800/100 800/100 800/100 800/100 600/40 800/100 800/100 600/40 600/40 800/100 800/100 800/100 600/40 800/100 600/40 600/40 800/100 600/40 550/20; 800/100 550/20; 800/100 800/100 800/100 550/20 Epoch 2007.4871 2007.2493 2007.2494 2007.5090 2007.2493 2007.2437 2007.2493 2007.4872 2007.4873 2007.4872 2007.2493 2007.4872 2007.2493 2007.4901 2007.4901 2007.4901 2007.4929 2007.4954 2007.4953 2007.4955 2007.5065 2007.5064 2007.5117 2007.5117 2007.4955 2007.5065 2007.5118 2007.4901 2007.5065 2007.5093 2007.5065 2007.4953 2007.5118 2007.5066 2007.5118 2007.4953 2007.5118 2007.5066 2007.5092 2007.5092 2007.5066 2007.5093 2007.5093 2007.5093 2007.5093 2007.4953 2007.5094 2007.5119 2007.4952 2007.5119 2007.5119 2007.5121 2007.5121 2007.2494


8

Rastegaev et al.: Sp eckle Interferometry of Metal-Poor Stars .I I

Table 4. Supplementary data on resolved stars
Name of the system/subsystem G76-21 02h 07h G89-14 12h G59-1 G63-46 13h 14h G135-16 16h G168-42 18h G141-47 G142-44 19h 23h G190-10 23h G28-43 23h G217-8 G130-7 23h --metallicities are adopted from t Coordinates (2000.0) 41m 13s 6 +09 46 . 22m 31s 5 +08 49 . 08m 54s 7 +21 47 . 39m 59s 6 +12 35 . 04m 01s 6 +22 31 . 19m 51s 7 +22 38 . 53m 16s 5 +10 37 . 38m 53s 2 +16 25 . 07m 59s 8 +41 51 . 09m 32s 9 +00 42 . 26m 32s 8 +60 37 . 45m 00s 1 +30 20 . he CLLA catalog m
V

[m/H] -2.28 -1.90 -1.14 -1.03 -1.04 -1.42 -1.34 -1.17 -1.92 -1.80 -2.24 -1.62 1994).

12 10.17 13 10.40 19 9.49 22 9.37 30 10.16 20 11.51 26 10.5 34 11.16 20 11.22 40 9.96 43 10.47 10 11.72 (Carney et al.,

Total number of components 2 4 3 2 2 2 2 2 3 2 2 2


Rastegaev et al.: Sp eckle Interferometry of Metal-Poor Stars .I I

9

Table 5: WDS components for the stars of the sample Name WDS companion 00437+7211OSO 10AB 00437+7211OSO 10AC 12089+2147HDS1714Aa 0.3 12089+2147LDS 930AB 15.7 13360+0112OSO 54 13400+1235HDS1917 0.2 14189+7314OSO 55AB 14189+7314OSO 55AC 15144+3301OSO 62 15307+0824OSO 64 16032+4215OSO 67 16199+2238OSO 68AB 16199+2238OSO 68AC 16283+4441OSO 71 16325-0834OSO 72 16348-0412GIC 144AB 1170.7 16348-0412LMP 14AC 16348-0412LMP 14BD 16348-0412LMP 14BE 16502+2219OSO 74AB 16502+2219OSO 74AC 17260-0245OSO 78AB 17260-0245OSO 78AC 17398+0225OSO 83AB 17398+0225OSO 83AC 17475-0847OSO 84AB 17475-0847OSO 84AC 17475-0847OSO 84AD 17523+3624OSO 85 17530+1521OSO 86AB 17530+1521OSO 86AC 17547+2016OSO 88 17551+3745OSO 89AB 17551+3745OSO 89AC 17551+3745OSO 89AD 18079+0153OSO 93AB 18079+0153OSO 93AC 18079+0153OSO 93AD 18079+0153OSO 93AE 18079+0153OSO 93AF 18115+1455OSO 94 18124+0524OSO 95 18353+2842OSO 101AB 18353+2842OSO 101AC 18353+2842OSO 101AD 18353+2842OSO 101AE 18353+2842OSO 101AF 19297+0102OSO 109AB 19297+0102OSO 109AC 19297+0102OSO 109AD 19297+0102OSO 109AE 19297+0102OSO 109AF 19297+0102OSO 109AG 19297+0102OSO 109AH ( ) m Status References - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) + (Perryman, 1997), + (Allen et al., 2000) - (Zapatero Osorio & Martin, 2004) + (Perryman, 1997), - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) + (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) ? - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - - - - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) ? - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) ? ? - (Zapatero Osorio & Martin, 2004) ? -?

G242-65 G59-1 G62-52 G63-46 G239-12 G1 G1 G1 G1 7 5 8 6 9-2 0822 4 24 42

2.25 5.51 0.68

G180-58 G153-64 G17-25

4.25

G169-28 G19-25 G20-8 G20-15

G182-31 G183-9 G183-11 G182-32

G20-24

G140-44 G140-46 G206-34

G92-6


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Rastegaev et al.: Sp eckle Interferometry of Metal-Poor Stars .I I

Table 5: WDS components of the stars of the sample (Contd.) Name WDS compani 19297+0102OSO 109AI 19297+0102OSO 109AJ 19297+0102OSO 109AK G142-44 19389+1626OSO 110AB 19389+1626OSO 110AC 19389+1626OSO 110AD 19389+1626OSO 110AE 19389+1626OSO 110AF 19389+1626OSO 110AG 19389+1626OSO 110AH 20248+2503OSO 125AB G186-26 20248+2503OSO 125AC G210-33 20454+4023OSO 133AB 20454+4023OSO 133AC 20454+4023OSO 133AD 20454+4023OSO 133AE 20553+4218OSO 137AB G212-7 20553+4218OSO 137AC 20553+4218OSO 137AD 20553+4218OSO 137AE 20553+4218OSO 137AF 20553+4218OSO 137AG G187-40 21220+2727OSO 145 G93-27 21399+0623OSO 151AB 21399+0623OSO 151AC G231-52 21393+6017OSO 150 21440+2723OSO 155 G188-22 G188-30 21553+3239OSO 162AB 21553+3239OSO 162AC 21554+5608OSO 163AB G232-40 21554+5608OSO 163AC G214-5 21592+4102OSO 164AB 21592+4102OSO 164AC 21592+4102OSO 164AD 22032-0113LDS4938AB G27-8 22032-0113OSO 166AC G126-62 22115+1806CHR 119Aa,Ab 22115+1806OSO 171Aa,B LFT 1697 22144-0845OSO 174 G18-39 22186+0827OSO 175 22328-0557OSO 181 G27-33 G233-26 22399+6143OSO 184AB 22399+6143OSO 184AC 23080+4151OSO 189 G190-10 G217-8 23265+6038OSO 196AB 23265+6038OSO 196AC 23265+6038OSO 196AD 23265+6038OSO 196AE 23450+3020OSO 204 G130-7 G29-71 23500+0843OSO 207 on ( ) m Status Reference ? - (Zapatero Osorio & Martin, 2004) ? - - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) -? - (Zapatero Osorio & Martin, 2004) ? -? - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) ? - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) + (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) + (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) -? ? +? - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004) - (Zapatero Osorio & Martin, 2004)

3.3

2.66

5.0

6.93

0.2